- ID:
- ivo://CDS.VizieR/J/A+A/597/A48
- Title:
- Stellar kinematics in CALIFA survey
- Short Name:
- J/A+A/597/A48
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the stellar kinematic maps of a large sample of galaxies from the integral-field spectroscopic survey CALIFA. The sample comprises 300 galaxies displaying a wide range of morphologies across the Hubble sequence, from ellipticals to late-type spirals. This dataset allows us to homogeneously extract stellar kinematics up to several effective radii. In this paper, we describe the level of completeness of this subset of galaxies with respect to the full CALIFA sample, as well as the virtues and limitations of the kinematic extraction compared to other well-known integral-field surveys. In addition, we provide averaged integrated velocity dispersion radial profiles for different galaxy types, which are particularly useful to apply aperture corrections for single aperture measurements or poorly resolved stellar kinematics of high-redshift sources. The work presented in this paper sets the basis for the study of more general properties of galaxies that will be explored in subsequent papers of the survey.
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/J/A+AS/133/317
- Title:
- Stellar kinematics in spiral galaxies
- Short Name:
- J/A+AS/133/317
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the results of absorption spectroscopy on the inner region of 34 Sa-Sc galaxies. We have determined the central velocity dispersion and, for 32 of these objects, stellar rotation curves and velocity-dispersion profiles. Some of these profiles are limited to the bulge, some others do reach a region dominated by the luminosity of the disk. These data are intended to provide basic material for the study of the mass distribution and dynamical status in the central regions of spiral galaxies. Although no elaborate bulge-and-disk photometric decomposition is performed, we estimate the effects of limited resolution and contamination by disk light on the central velocity dispersion of the bulge.
- ID:
- ivo://CDS.VizieR/J/A+AS/136/509
- Title:
- Stellar kinematics in spiral galaxies. II.
- Short Name:
- J/A+AS/136/509
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a second dataset of absorption spectroscopy on the inner region of spiral galaxies. We have determined the central velocity dispersion for 42 Sa-Sc objects and, for 32 of them, stellar rotation curves and velocity-dispersion profiles. Some of these profiles are limited to the bulge, some others do reach a region dominated by the luminosity of the disk. These data are intended to provide basic material for the study of the mass distribution and dynamical status in the central regions of spiral galaxies. Although no elaborate bulge-and-disk photometric decomposition is performed, we estimate the effects of limited resolution and contamination by disk light on the central velocity dispersion of the bulge. All the material presented in this paper, in particular the spectra, is available on-line.
- ID:
- ivo://CDS.VizieR/J/MNRAS/401/1521
- Title:
- Stellar masses of Lyman break galaxies at z~3
- Short Name:
- J/MNRAS/401/1521
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present results of a large survey of the mid-infrared (mid-IR) properties of 248 Lyman Break Galaxies (LBGs) with confirmed spectroscopic redshift using deep Spitzer/Infrared Array Camera (IRAC) observations in six cosmological fields. By combining the new mid-IR photometry with optical and near-infrared observations, we model the spectral energy distributions (SEDs) employing a revised version of the Bruzual and Charlot synthesis population code that incorporates a new treatment of the thermal-pulsating asymptotic giant branch phase (CB07). Our primary aim is to investigate the impact of the AGB phase in the stellar masses of the LBGs, and compare our new results with previous stellar mass estimates. We investigate the stellar mass of the LBG population as a whole and assess the benefits of adding longer wavelengths to estimates of stellar masses for high-redshift galaxies.
- ID:
- ivo://CDS.VizieR/J/ApJ/819/L27
- Title:
- Stellar masses of optical & IR QSO hosts
- Short Name:
- J/ApJ/819/L27
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The relation between star formation rates (SFRs) and stellar masses, i.e., the galaxy main sequence, is a useful diagnostic of galaxy evolution. We present the distributions relative to the main sequence of 55 optically selected PG and 12 near-IR-selected Two Micron All Sky Survey (2MASS) quasars at z<=0.5. We estimate the quasar host stellar masses from Hubble Space Telescope or ground-based AO photometry, and the SFRs through the mid-infrared aromatic features and far-IR photometry. We find that PG quasar hosts more or less follow the main sequence defined by normal star-forming galaxies while 2MASS quasar hosts lie systematically above the main sequence. PG and 2MASS quasars with higher nuclear luminosities seem to have higher specific SFRs (sSFRs), although there is a large scatter. No trends are seen between sSFRs and SMBH masses, Eddington ratios, or even morphology types (ellipticals, spirals, and mergers). Our results could be placed in an evolutionary scenario with quasars emerging during the transition from ULIRGs/mergers to ellipticals. However, combined with results at higher redshift, they suggest that quasars can be widely triggered in normal galaxies as long as they contain abundant gas and have ongoing star formation.
- ID:
- ivo://CDS.VizieR/J/ApJ/675/234
- Title:
- Stellar mass functions for galaxies 0<z<4
- Short Name:
- J/ApJ/675/234
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Using a sample of ~28000 sources selected at 3.6-4.5um with Spitzer observations of the Hubble Deep Field North, the Chandra Deep Field South, and the Lockman Hole (surveyed area ~664arcmin^2^), we study the evolution of the stellar mass content of the universe at 0<z<4. We calculate stellar masses and photometric redshifts, based on ~2000 templates built with stellar population and dust emission models fitting the ultraviolet to mid-infrared spectral energy distributions of galaxies with spectroscopic redshifts. We estimate stellar mass functions for different redshift intervals.
- ID:
- ivo://CDS.VizieR/J/ApJ/777/18
- Title:
- Stellar mass functions of galaxies to z=4
- Short Name:
- J/ApJ/777/18
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present measurements of the stellar mass functions (SMFs) of star-forming and quiescent galaxies to z=4 using a sample of 95675 K_s_-selected galaxies in the COSMOS/UltraVISTA field (Muzzin et al. 2013ApJS..206....8M). The SMFs of the combined population are in good agreement with previous measurements and show that the stellar mass density of the universe was only 50%, 10%, and 1% of its current value at z~0.75, 2.0, and 3.5, respectively. The quiescent population drives most of the overall growth, with the stellar mass density of these galaxies increasing as {rho}_star_{prop.to}(1+z)^-4.7+/-0.4^ since z=3.5, whereas the mass density of star-forming galaxies increases as {rho}_star_{prop.to}(1+z)^-2.3 +/-0.2^. At z>2.5, star-forming galaxies dominate the total SMF at all stellar masses, although a non-zero population of quiescent galaxies persists to z=4. Comparisons of the K_s_-selected star-forming galaxy SMFs with UV-selected SMFs at 2.5<z<4 show reasonable agreement and suggest that UV-selected samples are representative of the majority of the stellar mass density at z>3.5. We estimate the average mass growth of individual galaxies by selecting galaxies at fixed cumulative number density. The average galaxy with log(M_star_/M_{sun}_)=11.5 at z=0.3 has grown in mass by only 0.2dex (0.3dex) since z=2.0 (3.5), whereas those with log(M_star_/M_{sun}_)=10.5 have grown by >1.0dex since z=2. At z<2, the time derivatives of the mass growth are always larger for lower-mass galaxies, which demonstrates that the mass growth in galaxies since that redshift is mass-dependent and primarily bottom-up. Lastly, we examine potential sources of systematic uncertainties in the SMFs and find that those from photo-z templates, stellar population synthesis modeling, and the definition of quiescent galaxies dominate the total error budget in the SMFs.
- ID:
- ivo://CDS.VizieR/J/ApJ/633/844
- Title:
- Stellar mass in disk-dominated galaxies
- Short Name:
- J/ApJ/633/844
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We investigate the correlations among stellar mass (M*), disk scale length (R_d_), and rotation velocity at 2.2 disk scale lengths (V_2.2_) for a sample of 81 disk-dominated galaxies (disk/total>=0.9) selected from the SDSS. We measure V_2.2_ from long-slit H{alpha} rotation curves and infer M* from galaxy i-band luminosities (L_i_) and g-r colors.
- ID:
- ivo://CDS.VizieR/J/ApJ/856/15
- Title:
- Stellar mass-metallicity relation. I.
- Short Name:
- J/ApJ/856/15
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the stellar mass-stellar metallicity relationship (MZR) in the galaxy cluster Cl0024+1654 at z~0.4 using full-spectrum stellar population synthesis modeling of individual quiescent galaxies. The lower limit of our stellar mass range is M*=10^9.7^M_{sun}_, the lowest galaxy mass at which individual stellar metallicity has been measured beyond the local universe. We report a detection of an evolution of the stellar MZR with observed redshift at 0.037+/-0.007dex per Gyr, consistent with the predictions from hydrodynamical simulations. Additionally, we find that the evolution of the stellar MZR with observed redshift can be explained by an evolution of the stellar MZR with the formation time of galaxies, i.e., when the single stellar population (SSP)-equivalent ages of galaxies are taken into account. This behavior is consistent with stars forming out of gas that also has an MZR with a normalization that decreases with redshift. Lastly, we find that over the observed mass range, the MZR can be described by a linear function with a shallow slope ([Fe/H]{propto}(0.16+/-0.03)logM*). The slope suggests that galaxy feedback, in terms of mass-loading factor, might be mass-independent over the observed mass and redshift range.
- ID:
- ivo://CDS.VizieR/J/MNRAS/506/928
- Title:
- Stellar mass-size relation for low M* galaxies
- Short Name:
- J/MNRAS/506/928
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We reliably extend the stellar mass-size relation over 0.2<=z<=2 to low stellar mass galaxies by combining the depth of Hubble Frontier Fields (HFF) with the large volume covered by CANDELS. Galaxies are simultaneously modelled in multiple bands using the tools developed by the MegaMorph project, allowing robust size (i.e., half-light radius) estimates even for small, faint, and high redshift galaxies. We show that above 10^7^M_{sun}_, star-forming galaxies are well represented by a single power law on the mass-size plane over our entire redshift range. Conversely, the stellar mass - size relation is steep for quiescent galaxies with stellar masses >=10^10.3^M_{sun}_ and flattens at lower masses, regardless of whether quiescence is selected based on star-formation activity, rest-frame colours, or structural characteristics. This flattening occurs at sizes of ~1kpc at z<=1. As a result, a double power law is preferred for the stellar mass-size relation of quiescent galaxies, at least above 10^7^M_{sun}_. We find no strong redshift dependence in the slope of the relation of star-forming galaxies as well as of high mass quiescent galaxies. We also show that star-forming galaxies with stellar masses >=10^9.5^M_{sun}_ and quiescent galaxies with stellar masses>=10^10.3^M_{sun}_ have undergone significant size growth since z~2, as expected; however, low mass galaxies have not. Finally, we supplement our data with predominantly quiescent dwarf galaxies from the core of the Fornax cluster, showing that the stellar mass-size relation is continuous below 10^7^M_{sun}_, but a more complicated functional form is necessary to describe the relation.
